Pith. sign in

REVIEW 2 major objections 5 minor 96 references

Neutrino flux from WIMP annihilation around primordial black holes caps their dark-matter fraction at a few times 10^{-5} and the small-scale curvature power at about 10^{-1.65}.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · grok-4.5

2026-07-14 11:03 UTC pith:UVYKXAB6

load-bearing objection Clean multi-channel extension of UCMH-neutrino limits that also maps to P_R; useful complementary numbers, not a paradigm shift. the 2 major comments →

arxiv 2607.10524 v1 pith:UVYKXAB6 submitted 2026-07-12 astro-ph.CO

Constraining primordial black holes and primordial curvature power spectrum with extragalactic muon neutrino

Yupeng Yang This is my paper
classification astro-ph.CO
keywords primordial black holesWIMPsultracompact minihalosextragalactic neutrinosIceCubeprimordial curvature power spectrummixed dark matter
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper asks how much of the dark matter can be primordial black holes if the rest is ordinary WIMPs that pile up around them. After each black hole forms, WIMPs accrete into dense ultracompact minihalos whose annihilation rate is far higher than in ordinary galactic halos. The resulting extragalactic muon-neutrino flux is calculated for three annihilation channels and two IceCube event classes (contained and upward-going). Requiring that flux not exceed the measured atmospheric neutrino background for a one-year exposure yields upper limits on the PBH fraction. The tightest bound is f_PBH ~ 4 imes10^{-5} for 1 TeV WIMPs annihilating directly to muon neutrinos around 10^3 solar-mass black holes. That abundance limit is then converted, via the standard Press-Schechter mapping, into an upper bound on the primordial curvature power spectrum of order 10^{-1.65} at wave-numbers around 3 imes10^{12} Mpc^{-1}. The result supplies an independent neutrino-based check on small-scale primordial fluctuations that is complementary to gamma-ray and CMB constraints.

Core claim

For a mixed WIMP-plus-PBH dark-matter cosmology, the extragalactic muon-neutrino flux produced by WIMP annihilation inside the ultracompact minihalos that form around PBHs cannot exceed the atmospheric neutrino background. The strongest one-year IceCube limit obtained from this requirement is f_PBH ~ 4 imes10^{-5} (upward events, u_ u¯ channel, m_ u = 10^3 GeV, M_PBH = 10^3 M_ u). Mapping that abundance limit through the Press-Schechter formalism yields P_R ~ 10^{-1.65} at k ~ 3 imes10^{12} Mpc^{-1}.

What carries the argument

The piecewise WIMP density profile inside each ultracompact minihalo (inner r^{-3/4}, intermediate r^{-3/2}, outer r^{-9/4}, capped by the annihilation density ho_max). The square of this profile enters the neutrino luminosity, so the entire f_PBH and P_R limits scale directly with the assumed cusp strength.

Load-bearing premise

The calculation treats the multi-power-law density profile of WIMPs around every primordial black hole, fixed by kinetic-decoupling temperature and a hard annihilation cap, as exact; any softening of that cusp would weaken the neutrino signal and the derived limits.

What would settle it

A one-year IceCube analysis that isolates the high-energy muon sample and finds an excess (or a tighter null result) above atmospheric background in the energy window set by a 1 TeV WIMP annihilating to u_ u¯ would directly confirm or rule out the quoted f_PBH ~ 4 imes10^{-5} bound.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • For PBH masses above roughly 10^{-11} M_ u the neutrino limits become nearly mass-independent, so the same f_PBH ceiling applies across a wide intermediate-mass window.
  • The corresponding P_R bound is stronger than pure-PBH limits over 10^7 ≲ k ≲ 10^{13} Mpc^{-1}, tightening the allowed amplitude of small-scale primordial fluctuations.
  • Direct annihilation to muon neutrinos yields the strongest constraint; other channels (μ^+μ^-, τ^+τ^-) give limits weaker by factors of a few to ten.
  • Upward-going events generally out-perform contained events once the WIMP mass is high enough for long muon tracks, reversing the hierarchy seen at lower mass.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If future multi-year IceCube or KM3NeT exposures improve the high-energy atmospheric background subtraction by even a factor of a few, the same minihalo calculation would push f_PBH into the 10^{-6} range and P_R correspondingly lower.
  • Because the neutrino limits are still four orders of magnitude weaker than isotropic gamma-ray bounds on the same minihalos, a joint gamma-plus-neutrino analysis could test whether the density-profile assumptions are consistent across messengers.
  • The same UCMH luminosity that produces the neutrino flux also sources high-energy electrons and positrons; a parallel AMS-02 or future space-based positron bound would provide an independent cross-check of the annihilation rate used here.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

2 major / 5 minor

Summary. The paper studies a mixed WIMP+PBH dark-matter scenario in which WIMPs accrete onto PBHs to form UCMHs with the piecewise density profile of Eq. (1) (capped by the annihilation density of Eq. (5)). It computes the extragalactic muon-neutrino flux from WIMP annihilation (Eq. (7)) for the channels μ⁺μ⁻, τ⁺τ⁻ and νμν̄μ, converts the flux into contained and upward muon events via the standard formulae (8)–(11), and obtains 2σ upper limits on f_PBH by requiring that the signal not exceed the atmospheric-neutrino background for a one-year IceCube exposure (Eq. (14)). The strongest limits are f_PBH ∼ 10^{-4} (4 imes10^{-5}) for contained (upward) events at m_χ = 10^3 GeV and M_PBH = 10^3 M_⊙ in the νμν̄μ channel. These bounds are then mapped, via the Gaussian Press–Schechter relation, onto upper limits on the primordial curvature power spectrum, reaching P_R ∼ 10^{-1.65} at k ∼ 3 imes10^{12} Mpc^{-1}.

Significance. If the adopted UCMH density profile is accepted, the work supplies a clean, complementary neutrino-based bound on mixed WIMP+PBH dark matter that extends previous μ⁺μ⁻-only analyses to three channels and a wider PBH mass range, and that improves existing P_R limits over 10^7 ≲ k ≲ 10^{13} Mpc^{-1}. The calculation is fully standard once the profile is fixed, the comparison with an independently measured atmospheric background is free of circularity, and the results are directly falsifiable with IceCube data. The explicit conversion of the f_PBH limits into P_R constraints further increases the paper’s utility for early-universe cosmology.

major comments (2)
  1. The entire set of f_PBH and P_R limits rests on the piecewise density profile of Eq. (1) (with transition radii fixed by the kinetic-decoupling parameters of Eqs. (2)–(4) and the hard annihilation cap of Eq. (5)). While this profile is taken from the literature, no quantitative assessment is given of how the annihilation luminosity (and therefore the quoted limits) changes if the inner cusp is softened, if T_KD is varied within its theoretical uncertainty, or if a different ho_max prescription is used. A short sensitivity study or an explicit statement of the scaling of the luminosity with these parameters is needed before the strongest numerical claims can be regarded as robust.
  2. Section 3.2 adopts energy-independent effective volume V_eff = 0.04 km^{3} and area A_eff = 1 km^{2} for IceCube. Because the muon spectrum hardens with m_χ and the atmospheric background falls steeply, an energy-dependent acceptance would shift the relative strength of the contained versus upward limits and could alter the quoted best-case numbers by a non-negligible factor. Either a justification that the constant approximation is adequate at the energies of interest or a recalculation with published IceCube effective areas is required.
minor comments (5)
  1. The abstract and the final paragraph of Sec. 3.2 both state that the strongest limits come from the νμν̄μ channel, yet Fig. 2 shows that for m_χ = 10^{2} GeV the contained-event limits from μ⁺μ⁻ are competitive; a brief clarifying sentence would avoid confusion.
  2. The assumption of a monochromatic PBH mass function is never stated explicitly; a short remark in Sec. 3 or 4 would make the scope of the P_R bounds clearer.
  3. Several typographical issues appear (missing spaces after commas, inconsistent use of “WIMPs” vs “WIMP”, and the repeated reference “[17, 17, 18]”). A careful proof-reading pass is recommended.
  4. Figure 1 caption should specify that the curves assume f_PBH = 1; the body text does so, but the caption does not.
  5. The 1:1:1 flavor ratio after oscillation is adopted without citation or discussion of possible deviations for the direct νμν̄μ channel; a one-sentence reference would suffice.

Circularity Check

0 steps flagged

No circularity: f_PBH limits are standard flux-vs-external-ATM upper bounds; P_R follows from literature Press-Schechter conversion.

full rationale

The derivation chain is self-contained and non-circular. The neutrino flux (Eq. 7) is linear in f_PBH; the muon rates (Eqs. 8, 10) and event counts (Eq. 13) are computed from that flux using fixed literature inputs (DarkSUSY spectra, canonical ⟨σv⟩, energy-independent V_eff/A_eff, 1:1:1 flavor ratio). Upper limits on f_PBH are then obtained by the ordinary statistical requirement that the predicted signal not exceed the independently measured atmospheric background (Eq. 12) via the ζ statistic (Eq. 14). The subsequent conversion to P_R uses the standard Gaussian Press-Schechter formulae (Eqs. 15–19) with literature values of δ_c; no parameter is fitted to the same data that is later “predicted.” Self-citations (e.g., to the author’s earlier muon-neutrino paper) supply only the prior context that is being extended; they are not load-bearing uniqueness theorems or ansatzes that force the present numerical results. The piecewise UCMH density profile (Eq. 1) is an external modeling assumption taken from the literature, not a circular definition. Consequently the claimed bounds do not reduce to their inputs by construction.

Axiom & Free-Parameter Ledger

5 free parameters · 4 axioms · 0 invented entities

The central numerical claims rest on a chain of standard cosmological and particle-physics assumptions plus a handful of fixed experimental and theoretical parameters taken from the literature; no new free functions are fitted to data, but several conventional choices (〈σv〉, δ_c, effective volume) directly set the quoted numbers.

free parameters (5)
  • 〈σv〉 = 3×10^{-26} cm^{3} s^{-1}
    Canonical thermal value 3×10^{-26} cm^{3} s^{-1} fixes ρ_max and therefore the annihilation luminosity of every UCMH.
  • V_eff / A_eff = 0.04 km^{3} / 1 km^{2}
    Energy-independent IceCube effective volume 0.04 km^{3} and area 1 km^{2} convert differential fluxes into event counts.
  • E_th^μ = 50 GeV
    Muon energy threshold of 50 GeV enters the range integral R(E_μ) for upward events.
  • δ_c = 0.42 (fiducial)
    Critical density contrast for PBH formation (0.42 / 0.66 / 1/3) controls the conversion from f_PBH to P_R.
  • γ, g_*i = 0.2, ≈100
    Collapse fraction γ=0.2 and relativistic degrees of freedom g_*i≈100 fix the β–f_PBH relation (Eq. 19).
axioms (4)
  • domain assumption WIMP density profile inside a UCMH follows the three-segment power law of Eq. (1) with transitions fixed by kinetic decoupling.
    Taken from Eroshenko, Boucenna et al. and subsequent works; any deviation in the inner cusp directly rescales the annihilation rate.
  • domain assumption Primordial density perturbations are Gaussian and the Press-Schechter formalism with a top-hat window applies.
    Used without modification to convert β(M) into P_R (Eqs. 15–18).
  • domain assumption Neutrino flavor ratio at Earth is exactly 1:1:1 and atmospheric neutrinos are the sole background.
    Simplifies the conversion from source spectrum to detected muon flux; stated in Sec. 3.1.
  • standard math Standard ΛCDM expansion history and radiation-matter equality density ρ_eq.
    Enters the redshift integral of the extragalactic flux (Eq. 7).

pith-pipeline@v1.1.0-grok45 · 23624 in / 3028 out tokens · 45044 ms · 2026-07-14T11:03:46.281995+00:00 · methodology

0 comments
read the original abstract

We investigate a mixed dark matter scenario comprising weakly interacting massive particles (WIMPs) and primordial black holes (PBHs). After PBH formation, WIMPs can accrete onto them, forming ultracompact minihalos (UCMHs). The resulting WIMP number density within UCMHs is significantly enhanced compared to classical dark matter halo models, leading to a higher WIMP annihilation rate. Previous studies have focused mainly on the associated gamma-ray flux, we investigate the extragalactic neutrino flux from such annihilation. Considering the annihilation channels $\mu^{+}\mu^{-}$, $\tau^{+}\tau^{-}$, and $\nu_{\mu}\bar{\nu}_{\mu}$, we analyze two classes of neutrino events: upward and contained events. By requiring the neutrino flux from WIMP annihilation around PBHs does not exceed the atmospheric neutrino background, we derive upper limits on the fraction of dark matter in PBHs ($f_{\rm PBH}$) for a one-year exposure of the IceCube experiment. These limits depend on the annihilation channel, the masses of the WIMP and PBH, and the neutrino event type. The strongest constraints come from the $\nu_{\mu}\bar{\nu}_{\mu}$ channel, yielding $f_{\rm PBH} \sim 10^{-4}$ ($4\times 10^{-5}$) for contained (upward) events with $m_{\chi}=10^{3}$ GeV and $M_{\rm PBH}=10^{3} M_{\odot}$. Based on these bounds on PBHs, we further derive upper limits on the primordial curvature power spectrum $\mathcal{P}_{\mathcal{R}}$. From our strongest constraint, we obtain $\mathcal{P}_{\mathcal{R}} \sim 10^{-1.65}$ at the scale $k\sim 3\times 10^{12}~\mathrm{Mpc^{-1}}$.

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

96 extracted references · 26 canonical work pages · 19 internal anchors

  1. [1]

    Roszkowski, Particle dark matter: A Theorist’s perspec- tive

    L. Roszkowski, Particle dark matter: A Theorist’s perspec- tive. Pramana 62, 389–401 (2004).https://doi.org/10. 1007/BF02705097. arXiv:hep-ph/0404052

    Pith/arXiv arXiv 2004

  2. [2]

    Schumann, Direct Detection of WIMP Dark Mat- ter: Concepts and Status

    M. Schumann, Direct Detection of WIMP Dark Mat- ter: Concepts and Status. J. Phys. G 46(10), 103003 (2019). https://doi.org/10.1088/1361-6471/ab2ea5. arXiv:1903.03026 [astro-ph.CO]

    Pith/arXiv arXiv doi:10.1088/1361-6471/ab2ea5 2019

  3. [3]

    Bertone, D

    G. Bertone, D. Hooper, J. Silk, Particle dark matter: evidence, candidates and constraints. Phys.Rept 405(5- 6), 279–390 (2005).https://doi.org/10.1016/j.physrep. 2004.08.031. arXiv:hep-ph/0404175 [hep-ph]

    Pith/arXiv arXiv doi:10.1016/j.physrep 2005

  4. [4]

    Dark Matter in Astrophysics/Cosmology

    A.M. Green, Dark Matter in Astrophysics/Cosmology. Sci- Post Phys. Lect. Notes arXiv:2109.05854 (2021). https: //doi.org/10.48550/arXiv.2109.05854. arXiv:2109.05854 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2109.05854 2021

  5. [5]

    Jungman, M

    G. Jungman, M. Kamionkowski, K. Griest, Supersymmet- ric dark matter. Phys.Rept 267, 195–373 (1996).https: //doi.org/10.1016/0370-1573(95)00058-5. arXiv:hep- ph/9506380 [hep-ph]

    doi:10.1016/0370-1573(95)00058-5 1996

  6. [6]

    Aprile, et al., Dark Matter Search Results from a One Ton-Year Exposure of XENON1T

    E. Aprile, et al., Dark Matter Search Results from a One Ton-Year Exposure of XENON1T. Phys. Rev. Lett. 121(11), 111302 (2018). https://doi.org/10.1103/ PhysRevLett.121.111302. arXiv:1805.12562 [astro-ph.CO]

    Pith/arXiv arXiv 2018

  7. [7]

    Arcadi, M

    G. Arcadi, M. Dutra, P. Ghosh, M. Lindner, Y. Mambrini, M. Pierre, S. Profumo, F.S. Queiroz, The waning of the WIMP? A review of models, searches, and constraints. Eur. Phys. J. C 78(3), 203 (2018). https://doi.org/10.1140/ epjc/s10052-018-5662-y. arXiv:1703.07364 [hep-ph]

    Pith/arXiv arXiv 2018

  8. [8]

    Sci- Post Phys

    J.L.Feng,TheWIMPparadigm:Themeandvariations. Sci- Post Phys. Lect. Notes71, 1 (2023).https://doi.org/10. 21468/SciPostPhysLectNotes.71. arXiv:2212.02479 [hep- ph]

    Pith/arXiv arXiv 2023

  9. [9]

    B.J. Carr, K. Kohri, Y. Sendouda, J. Yokoyama, New cos- mological constraints on primordial black holes. Phys. Rev. D 81, 104019 (2010).https://doi.org/10.1103/PhysRevD. 81.104019. arXiv:0912.5297 [astro-ph.CO]

    Pith/arXiv arXiv doi:10.1103/physrevd 2010

  10. [10]

    Choi, E.D

    G. Choi, E.D. Schiappacasse, PBH assisted search for QCD axion dark matter. JCAP 09, 072 (2022). https://doi. org/10.1088/1475-7516/2022/09/072. arXiv:2205.02255 [hep-ph]

    Pith/arXiv arXiv doi:10.1088/1475-7516/2022/09/072 2022

  11. [14]

    Hertzberg, E.D

    M.P. Hertzberg, E.D. Schiappacasse, T.T. Yanagida, Im- plications for dark matter direct detection in the pres- ence of LIGO-motivated primordial black holes. Phys. Lett. B 807, 135566 (2020). https://doi.org/10.1016/ j.physletb.2020.135566. arXiv:1910.10575 [astro-ph.CO]

    arXiv 2020

  12. [15]

    B. Carr, K. Kohri, Y. Sendouda, J. Yokoyama, Con- straints on primordial black holes. Reports on Progress in Physics 84(11), 116902 (2021).https://doi.org/10.1088/ 1361-6633/ac1e31. arXiv:2002.12778 [astro-ph.CO]

    Pith/arXiv arXiv 2021

  13. [16]

    Bambi, Astrophysical Black Holes: A Review

    C. Bambi, Astrophysical Black Holes: A Review. PoS MUL TIF2019, 028 (2020). https://doi.org/10.22323/ 1.362.0028. arXiv:1906.03871 [astro-ph.HE]

    Pith/arXiv arXiv 2020

  14. [17]

    Hawking, Black hole explosions

    S.W. Hawking, Black hole explosions. Nature 248, 30–31 (1974). https://doi.org/10.1038/248030a0

    doi:10.1038/248030a0 1974

  15. [18]

    Hawking, Particle Creation by Black Holes

    S.W. Hawking, Particle Creation by Black Holes. Com- mun. Math. Phys. 43, 199–220 (1975).https://doi.org/ 10.1007/BF02345020. [Erratum: Commun.Math.Phys. 46, 206 (1976)]

    doi:10.1007/bf02345020 1975

  16. [19]

    Aghanim, et al., Planck 2018 results

    N. Aghanim, et al., Planck 2018 results. VI. Cosmologi- cal parameters. A&A 641, A6 (2020). https://doi.org/ 10.1051/0004-6361/201833910. arXiv:1807.06209 [astro- ph.CO]

    Pith/arXiv arXiv doi:10.1051/0004-6361/201833910 2018

  17. [20]

    Adamek, C.T

    J. Adamek, C.T. Byrnes, M. Gosenca, S. Hotchkiss, WIMPs and stellar-mass primordial black holes are incompatible. Phys. Rev. D 100(2), 023506 (2019). https://doi.org/ 10.1103/PhysRevD.100.023506. arXiv:1901.08528 [astro- ph.CO]

    Pith/arXiv arXiv doi:10.1103/physrevd.100.023506 2019

  18. [21]

    Constraining Mixed Dark-Matter Scenarios of WIMPs and Primordial Black Holes from CMB and 21-cm observations

    H. Tashiro, K. Kadota, Constraining mixed dark-matter scenarios of WIMPs and primordial black holes from CMB and 21-cm observations. Phys.Rev.D 103(12), 123532 (2021). https://doi.org/10.1103/PhysRevD.103.123532. arXiv:2104.09738 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.103.123532 2021

  19. [22]

    Berteaud, F

    J. Berteaud, F. Calore, J. Iguaz, P.D. Serpico, T. Siegert, Strong constraints on primordial black hole dark matter from 16 years of INTEGRAL/SPI observations. Phys. Rev. D 106(2), 023030 (2022).https://doi.org/10.1103/ PhysRevD.106.023030. arXiv:2202.07483 [astro-ph.HE] 8

    Pith/arXiv arXiv 2022

  20. [23]

    Z. Xie, B. Liu, J. Liu, Y.F. Cai, R. Yang, Limits on the primordial black holes dark matter with future MeV de- tectors. Phys. Rev. D 109(4), 043020 (2024). https:// doi.org/10.1103/PhysRevD.109.043020. arXiv:2401.06440 [astro-ph.HE]

    work page doi:10.1103/physrevd.109.043020 2024

  21. [24]

    Bernal, V

    N. Bernal, V. Muñoz-Albornoz, S. Palomares-Ruiz, P. Villanueva-Domingo, Current and future neutrino lim- its on the abundance of primordial black holes. JCAP10, 068 (2022). https://doi.org/10.1088/1475-7516/2022/ 10/068. arXiv:2203.14979 [hep-ph]

    Pith/arXiv arXiv doi:10.1088/1475-7516/2022/ 2022

  22. [25]

    Searching for Signal of Primordial Black Hole from CMB Lensing and $\gamma$-ray Emissions

    X.H. Tan, Y.J. Yan, T. Qiu, J.Q. Xia, Searching for the Signal of a Primordial Black Hole from CMB Lens- ing and γ-Ray Emissions. Astrophys. J. Lett. 939(1), L15 (2022). https://doi.org/10.3847/2041-8213/ac9668. arXiv:2209.15222 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/ac9668 2022

  23. [26]

    Facchinetti, M

    G. Facchinetti, M. Lucca, S. Clesse, Relaxing CMB bounds on primordial black holes: The role of ionization fronts. Phys. Rev. D 107(4), 043537 (2023). https://doi.org/ 10.1103/PhysRevD.107.043537. arXiv:2212.07969 [astro- ph.CO]

    Pith/arXiv arXiv doi:10.1103/physrevd.107.043537 2023

  24. [28]

    Poulin, P.D

    V. Poulin, P.D. Serpico, F. Calore, S. Clesse, K. Kohri, Cmb bounds on disk-accreting massive primordial black holes. Phys. Rev. D 96, 083524 (2017). https://doi.org/10. 1103/PhysRevD.96.083524. URL https://link.aps.org/ doi/10.1103/PhysRevD.96.083524

    doi:10.1103/physrevd.96.083524 2017

  25. [29]

    Auffinger, Primordial black hole constraints with Hawk- ing radiation—A review

    J. Auffinger, Primordial black hole constraints with Hawk- ing radiation—A review. Prog. Part. Nucl. Phys. 131, 104040 (2023). https://doi.org/10.1016/j.ppnp.2023. 104040. arXiv:2206.02672 [astro-ph.CO]

    Pith/arXiv arXiv doi:10.1016/j.ppnp.2023 2023

  26. [30]

    Khlopov, A

    M.Y. Khlopov, A. Barrau, J. Grain, Gravitino production by primordial black hole evaporation and constraints on the inhomogeneityoftheearlyuniverse. ClassicalandQuantum Gravity 23(6), 1875 (2006). https://doi.org/10.1088/ 0264-9381/23/6/004. URL https://dx.doi.org/10.1088/ 0264-9381/23/6/004

    2006

  27. [31]

    S. Jung, T. Kim, Gamma-ray burst lensing parallax: Clos- ing the primordial black hole dark matter mass window. Phys. Rev. Res.2(1), 013113 (2020).https://doi.org/10. 1103/PhysRevResearch.2.013113. arXiv:1908.00078 [astro- ph.CO]

    Pith/arXiv arXiv 2020

  28. [32]

    Mróz, et al., Limits on Planetary-mass Primordial Black Holes from the OGLE High-cadence Survey of the Magellanic Clouds

    P. Mróz, et al., Limits on Planetary-mass Primordial Black Holes from the OGLE High-cadence Survey of the Magellanic Clouds. Astrophys. J. Lett. 976(1), L19 (2024). https://doi.org/10.3847/2041-8213/ad8e68. arXiv:2410.06251 [astro-ph.CO]

    Pith/arXiv arXiv doi:10.3847/2041-8213/ad8e68 2024

  29. [33]

    B.Y. Su, X. Pan, G.S. Wang, L. Zu, Y. Yang, L. Feng, Constraining primordial black holes as dark matter using AMS-02 data. Eur. Phys. J. C84(6), 606 (2024). https: //doi.org/10.1140/epjc/s10052-024-12773-y. [Erratum: Eur.Phys.J.C 84, 768 (2024)]. arXiv:2403.04988 [astro- ph.HE]

    Pith/arXiv arXiv doi:10.1140/epjc/s10052-024-12773-y 2024

  30. [34]

    Yang, J.D

    C. Yang, J.D. Pan, X. Zhang, Constraining primordial black hole abundance with Insight-HXMT. Commun. Theor. Phys. 78(4), 045402 (2026). https://doi.org/10.1088/ 1572-9494/ae2583. arXiv:2412.09297 [astro-ph.CO]

    arXiv 2026

  31. [35]

    M.L. Zhao, S. Wang, X. Zhang, Prospects for probing dark matter particles and primordial black holes with the Hong- meng mission using the 21 cm global spectrum at cosmic dawn. JCAP 07, 039 (2025). https://doi.org/10.1088/ 1475-7516/2025/07/039. arXiv:2412.19257 [astro-ph.CO]

    Pith/arXiv arXiv 2025

  32. [36]

    J. Cang, Y. Gao, Y. Ma, Prospects of Future CMB Anisotropy Probes for Primordial Black Holes. JCAP05, 051 (2021). https://doi.org/10.1088/1475-7516/2021/ 05/051. arXiv:2011.12244 [astro-ph.CO]

    Pith/arXiv arXiv doi:10.1088/1475-7516/2021/ 2021

  33. [37]

    Zhang, B

    Z. Zhang, B. Yue, Y. Xu, Y.Z. Ma, X. Chen, M. Liu, Cos- mic radio background from primordial black holes at cos- mic dawn. Phys. Rev. D107(8), 083013 (2023). https:// doi.org/10.1103/PhysRevD.107.083013. arXiv:2303.06616 [astro-ph.CO]

    Pith/arXiv arXiv doi:10.1103/physrevd.107.083013 2023

  34. [38]

    G.W. Yuan, L. Lei, Y.Z. Wang, B. Wang, Y.Y. Wang, C. Chen, Z.Q. Shen, Y.F. Cai, Y.Z. Fan, Rapidly grow- ing primordial black holes as seeds of the massive high- redshift JWST Galaxies. Sci. China Phys. Mech. As- tron. 67(10), 109512 (2024). https://doi.org/10.1007/ s11433-024-2433-3. arXiv:2303.09391 [astro-ph.CO]

    Pith/arXiv arXiv 2024

  35. [39]

    Clark, B

    S. Clark, B. Dutta, Y. Gao, Y.Z. Ma, L.E. Strigari, 21 cm limits on decaying dark matter and primordial black holes. Phys. Rev. D98(4), 043006 (2018). https://doi.org/10. 1103/PhysRevD.98.043006. arXiv:1803.09390 [astro-ph.HE]

    Pith/arXiv arXiv 2018

  36. [40]

    Huang, Y.F

    J.Z. Huang, Y.F. Zhou, Constraints on evaporating primor- dial black holes from the AMS-02 positron data. Phys. Rev. D 111(8), 083525 (2025).https://doi.org/10.1103/ PhysRevD.111.083525. arXiv:2403.04987 [hep-ph]

    Pith/arXiv arXiv 2025

  37. [41]

    Boudaud, M

    M. Boudaud, M. Cirelli, Voyager 1e± Further Constrain Primordial Black Holes as Dark Matter. Phys. Rev. Lett. 122(4), 041104 (2019). https://doi.org/10.1103/ PhysRevLett.122.041104. arXiv:1807.03075 [astro-ph.HE]

    Pith/arXiv arXiv 2019

  38. [42]

    Yang, Constraints on primordial black holes and cur- vature perturbations from the global 21-cm signal

    Y. Yang, Constraints on primordial black holes and cur- vature perturbations from the global 21-cm signal. Phys. Rev. D 102(8), 083538 (2020).https://doi.org/10.1103/ PhysRevD.102.083538. arXiv:2009.11547 [astro-ph.CO]

    Pith/arXiv arXiv 2020

  39. [43]

    Yang, Influences of accreting primordial black holes on the global 21 cm signal in the dark ages

    Y. Yang, Influences of accreting primordial black holes on the global 21 cm signal in the dark ages. MNRAS 508(4), 5709–5715 (2021). https://doi.org/10.1093/ mnras/stab2966. arXiv:2110.06447 [astro-ph.CO]

    Pith/arXiv arXiv 2021

  40. [44]

    Constraints on accreting primordial black holes with the global 21-cm signal

    Y. Yang, Constraints on accreting primordial black holes with the global 21-cm signal. Phys. Rev. D104(6), 063528 (2021). https://doi.org/10.1103/PhysRevD.104.063528. arXiv:2108.11130 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.104.063528 2021

  41. [45]

    Yang, Impact of radiation from primordial black holes on the 21-cm angular-power spectrum in the dark ages

    Y. Yang, Impact of radiation from primordial black holes on the 21-cm angular-power spectrum in the dark ages. Phys. Rev.D 106(12),123508(2022). https://doi.org/10.1103/ PhysRevD.106.123508. arXiv:2209.00851 [astro-ph.CO]

    Pith/arXiv arXiv 2022

  42. [46]

    Eroshenko, Dark matter density spikes around pri- mordial black holes

    Y.N. Eroshenko, Dark matter density spikes around pri- mordial black holes. Astron. Lett. 42(6), 347–356 (2016). https://doi.org/10.1134/S1063773716060013. arXiv:1607.00612 [astro-ph.HE]

    Pith/arXiv arXiv doi:10.1134/s1063773716060013 2016

  43. [47]

    Constraints on primordial black holes with CMB spectral distortions

    Y. Yang, Constraints on primordial black holes with CMB spectral distortions. Phys.Rev.D 106(4), 043516 (2022). https://doi.org/10.1103/PhysRevD.106.043516. arXiv:2208.03458 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.106.043516 2022

  44. [49]

    Kadota, H

    K. Kadota, H. Tashiro, Primordial black hole dark mat- ter in the presence of p-wave WIMP annihilation. JCAP 03(03), 045 (2022).https://doi.org/10.1088/1475-7516/ 2022/03/045. arXiv:2112.04179 [astro-ph.CO]

    Pith/arXiv arXiv doi:10.1088/1475-7516/ 2022

  45. [50]

    Y. Yang, X. Li, G. Li, Constraints on primordial black holes in the mixed dark matter scenarios using the ratio ( 3He +D )/H. European Physical Journal C 83(10), 934 (2023). https://doi.org/10.1140/epjc/ s10052-023-12115-4. arXiv:2308.07010 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1140/epjc/ 2023

  46. [52]

    Boucenna, F

    S.M. Boucenna, F. Kuhnel, T. Ohlsson, L. Visinelli, Novel Constraints on Mixed Dark-Matter Scenarios of Primordial Black Holes and WIMPs. JCAP 07, 003 (2018). https://doi.org/10.1088/1475-7516/2018/07/

    work page doi:10.1088/1475-7516/2018/07/ 2018

  47. [53]

    arXiv:1712.06383 [hep-ph]

    Pith/arXiv arXiv

  48. [54]

    Boudaud, T

    M. Boudaud, T. Lacroix, M. Stref, J. Lavalle, P. Salati, In-depth analysis of the clustering of dark matter parti- cles around primordial black holes. Part I. Density pro- files. JCAP 08, 053 (2021). https://doi.org/10.1088/ 1475-7516/2021/08/053. arXiv:2106.07480 [astro-ph.CO]

    Pith/arXiv arXiv 2021

  49. [55]

    Ginés, O

    E.U. Ginés, O. Mena, S.J. Witte, Revisiting constraints on WIMPs around primordial black holes. Phys. Rev. D 106(6), 063538 (2022). https://doi.org/10.1103/ PhysRevD.106.063538. arXiv:2207.09481 [astro-ph.CO]

    Pith/arXiv arXiv 2022

  50. [56]

    Y. Yang, Q. Li, J. Hao, X. Li, Cosmological abundance of primordial black holes in mixed dark matter scenar- ios incorporating Kaluza–Klein dark matter. Int. J. Mod. Phys. D 34(13), 2550059 (2025). https://doi.org/10. 1142/S0218271825500592. arXiv:2506.20391 [astro-ph.CO]

    arXiv 2025

  51. [57]

    J. Hao, Y. Yang, Q. Li, Y. Qu, S. Yi, Muon neutrinos and the cosmological abundance of primordial black holes. Phys. Rev. D 110(2), 023532 (2024).https://doi.org/10.1103/ PhysRevD.110.023532. arXiv:2406.00664 [astro-ph.CO]

    Pith/arXiv arXiv 2024

  52. [58]

    Chanda, J

    P. Chanda, J. Scholtz, J. Unwin, Improved constraints on dark matter annihilations around primordial black holes. JHEP 07, 273 (2024). https://doi.org/10.1007/ JHEP07(2024)273. arXiv:2209.07541 [hep-ph]

    arXiv 2024

  53. [59]

    Navarro, C.S

    J.F. Navarro, C.S. Frenk, S.D.M. White, A Universal den- sity profile from hierarchical clustering. Astrophys. J. 490, 493–508 (1997). https://doi.org/10.1086/304888. arXiv:astro-ph/9611107

    Pith/arXiv arXiv doi:10.1086/304888 1997

  54. [60]

    Navarro, C.S

    J.F. Navarro, C.S. Frenk, S.D.M. White, The Structure of cold dark matter halos. Astrophys. J. 462, 563–575 (1996). https://doi.org/10.1086/177173. arXiv:astro- ph/9508025

    doi:10.1086/177173 1996

  55. [61]

    B. Carr, F. Kühnel, L. Visinelli, Black holes and WIMPs: all or nothing or something else. Mon. Not. Roy. Astron. Soc 506(3), 3648–3661 (2021).https://doi.org/10.1093/ mnras/stab1930. arXiv:2011.01930 [astro-ph.CO]

    Pith/arXiv arXiv 2021

  56. [62]

    Josan, A.M

    A.S. Josan, A.M. Green, K.A. Malik, Generalised con- straints on the curvature perturbation from primordial black holes. Phys. Rev. D79, 103520 (2009). https: //doi.org/10.1103/PhysRevD.79.103520. arXiv:0903.3184 [astro-ph.CO]

    Pith/arXiv arXiv doi:10.1103/physrevd.79.103520 2009

  57. [63]

    Hlozek, J

    R. Hlozek, J. Dunkley, G. Addison, J.W. Appel, J.R. Bond, C.S. Carvalho, S. Das, M.J. Devlin, R. Dünner, T. Essinger- Hileman, J.W. Fowler, P. Gallardo, A. Hajian, M. Halpern, M. Hasselfield, M. Hilton, A.D. Hincks, J.P. Hughes, K.D. Irwin, J. Klein, A. Kosowsky, T.A. Marriage, D. Marsden, F. Menanteau, K. Moodley, M.D. Niemack, M.R. Nolta, L.A. Page, L. ...

    2012

  58. [64]

    Bird, H.V

    S. Bird, H.V. Peiris, M. Viel, L. Verde, Minimally para- metric power spectrum reconstruction from the lyman α forest. Monthly Notices of the Royal Astronomical Soci- ety 413(3), 1717–1728 (2011).https://doi.org/10.1111/ j.1365-2966.2011.18245.x

    arXiv 2011

  59. [65]

    Tinker, E.S

    J.L. Tinker, E.S. Sheldon, R.H. Wechsler, M.R. Becker, E. Rozo, Y. Zu, D.H. Weinberg, I. Zehavi, M.R. Blanton, M.T. Busha, B.P. Koester, Cosmological constraints from galaxy clustering and the mass-to-number ratio of galaxy clusters. The Astrophysical Journal745(1), 16 (2012). URL http://stacks.iop.org/0004-637X/745/i=1/a=16

    2012

  60. [66]

    Ragavendra, A.K

    H.V. Ragavendra, A.K. Sarkar, S.K. Sethi, Constraining ul- traslowrollinflationusingcosmologicaldatasets. JCAP 07, 088 (2024). https://doi.org/10.1088/1475-7516/2024/ 07/088. arXiv:2404.00933 [astro-ph.CO]

    Pith/arXiv arXiv doi:10.1088/1475-7516/2024/ 2024

  61. [67]

    G.Sato-Polito,E.D.Kovetz,M.Kamionkowski,Constraints on the primordial curvature power spectrum from primor- dial black holes. Phys. Rev. D100, 063521 (2019). https: //doi.org/10.1103/PhysRevD.100.063521. URL https: //link.aps.org/doi/10.1103/PhysRevD.100.063521

    doi:10.1103/physrevd.100.063521 2019

  62. [68]

    Yang, Constraints on the small scale curvature pertur- bation using Planck-2015 data

    Y. Yang, Constraints on the small scale curvature pertur- bation using Planck-2015 data. Mon. Not. Roy. Astron. Soc. 486(4), 4569–4573 (2019).https://doi.org/10.1093/ mnras/stz1148. arXiv:1904.09104 [astro-ph.CO]

    Pith/arXiv arXiv 2015

  63. [69]

    Bringmann, P

    T. Bringmann, P. Scott, Y. Akrami, Improved constraints ontheprimordialpowerspectrumatsmallscalesfromultra- compactminihalos. Phys.Rev.D 85,125027(2012). https: //doi.org/10.1103/PhysRevD.85.125027. arXiv:1110.2484 [astro-ph.CO]

    Pith/arXiv arXiv doi:10.1103/physrevd.85.125027 2012

  64. [70]

    Scott, S

    P. Scott, S. Sivertsson, Gamma-Rays from Ultracompact Primordial Dark Matter Minihalos. Phys. Rev. Lett.103, 211301 (2009). https://doi.org/10.1103/PhysRevLett. 103.211301. [Erratum: Phys.Rev.Lett. 105, 119902 (2010)]. arXiv:0908.4082 [astro-ph.CO]

    Pith/arXiv arXiv doi:10.1103/physrevlett 2009

  65. [71]

    Y. Yang, G. Yang, H. Zong, Neutrino signals from ultracom- pact minihalos and constraints on the primordial curvature perturbation. Phys. Rev. D 87, 103525 (2013). https: //doi.org/10.1103/PhysRevD.87.103525. URL http:// link.aps.org/doi/10.1103/PhysRevD.87.103525

    work page doi:10.1103/physrevd.87.103525 2013

  66. [72]

    Y. Yang, L. Feng, X. Huang, X. Chen, T. Lu, H. Zong, Constraints on ultracompact minihalos from extragalactic γ-ray background. Journal of Cosmology and Astroparticle Physics 2011(12), 020–020 (2011). https://doi.org/10. 1088/1475-7516/2011/12/020. URL https://doi.org/10. 1088%2F1475-7516%2F2011%2F12%2F020

    2011

  67. [73]

    Y. Yang, X. Huang, X. Chen, H. Zong, New Constraints on Primordial Minihalo Abundance Using Cosmic Mi- crowaveBackgroundObservations. Phys.Rev.D 84,043506 (2011). https://doi.org/10.1103/PhysRevD.84.043506. arXiv:1109.0156 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.84.043506 2011

  68. [74]

    Emami, G.F

    R. Emami, G.F. Smoot, Observational constraints on the primordial curvature power spectrum. Journal of Cosmol- ogy and Astroparticle Physics 2018(01), 007–007 (2018). https://doi.org/10.1088/1475-7516/2018/01/007. URL http://dx.doi.org/10.1088/1475-7516/2018/01/007

    work page doi:10.1088/1475-7516/2018/01/007 2018

  69. [75]

    Y.P. Yang, X. Chen, T. Lu, H.S. Zong, The Abundance of New Kind of Dark Matter Structures. Eur. Phys. J. Plus 126, 123 (2011). https://doi.org/10.1140/epjp/ i2011-11123-8. arXiv:1112.6228 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1140/epjp/ 2011

  70. [76]

    Bertone, A.R

    G. Bertone, A.R. Zentner, J. Silk, New signature of dark matter annihilations: Gamma rays from intermediate-mass black holes. Phys. Rev. D 72, 103517 (2005). https: //doi.org/10.1103/PhysRevD.72.103517. URL https:// link.aps.org/doi/10.1103/PhysRevD.72.103517

    work page doi:10.1103/physrevd.72.103517 2005

  71. [77]

    Ullio, L

    P. Ullio, L. Bergstrom, J. Edsjo, C.G. Lacey, Cosmologi- cal dark matter annihilations into gamma-rays - a closer look. Phys. Rev. D 66, 123502 (2002). https://doi.org/ 10.1103/PhysRevD.66.123502. arXiv:astro-ph/0207125

    Pith/arXiv arXiv doi:10.1103/physrevd.66.123502 2002

  72. [78]

    Bringmann, J

    T. Bringmann, J. Edsjö, P. Gondolo, P. Ullio, L. Bergström, DarkSUSY 6 : An Advanced Tool to Compute Dark Mat- ter Properties Numerically. JCAP 07, 033 (2018). https://doi.org/10.1088/1475-7516/2018/07/033. arXiv:1802.03399 [hep-ph]

    Pith/arXiv arXiv doi:10.1088/1475-7516/2018/07/033 2018

  73. [79]

    Gondolo, J

    P. Gondolo, J. Edsjo, P. Ullio, L. Bergstrom, M. Schelke, E.A. Baltz, DarkSUSY: Computing supersymmetric dark 10 matter properties numerically. JCAP 07, 008 (2004). https://doi.org/10.1088/1475-7516/2004/07/008. arXiv:astro-ph/0406204

    Pith/arXiv arXiv doi:10.1088/1475-7516/2004/07/008 2004

  74. [80]

    Review of Neutrino Experiments Searching for Astrophysical Neutrinos

    V. Decoene, Review of Neutrino Experiments Searching for Astrophysical Neutrinos. PoSICRC2023, 026 (2023). https://doi.org/10.22323/1.444.0026. arXiv:2309.17139 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.22323/1.444.0026 2023

  75. [81]

    Gaisser, M

    T.K. Gaisser, M. Honda, Flux of atmospheric neutrinos. Annual Review of Nuclear and Particle Science 52, 153– 199 (2002). https://doi.org/10.1146/annurev.nucl.52. 050102.090645. arXiv:hep-ph/0203272 [hep-ph]

    work page doi:10.1146/annurev.nucl.52 2002

  76. [82]

    Status and prospects of the IceCube neutrino telescope

    E. Resconi, IceCube Collaboration, Status and prospects of the IceCube neutrino telescope. Nuclear Instruments and MethodsinPhysicsResearchA 602(1),7–13(2009). https: //doi.org/10.1016/j.nima.2008.12.013. arXiv:0807.3891 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.nima.2008.12.013 2009

  77. [83]

    Upward muon signals at neutrino detectors as a probe of dark matter properties

    J.Hisano,K.Nakayama,M.J.S.Yang,Upwardmuonsignals at neutrino detectors as a probe of dark matter properties. Physics Letters B 678(1), 101–106 (2009).https://doi. org/10.1016/j.physletb.2009.06.014. arXiv:0905.2075 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.physletb.2009.06.014 2009

  78. [84]

    Muon Fluxes From Dark Matter Annihilation

    A.E. Erkoca, M.H. Reno, I. Sarcevic, Muon fluxes from dark matter annihilation. Phys.Rev.D 80(4), 043514 (2009). https://doi.org/10.1103/PhysRevD.80.043514. arXiv:0906.4364 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.80.043514 2009

  79. [85]

    Strumia, F

    A. Strumia, F. Vissani, Neutrino masses and mixings and... arXiv e-prints hep-ph/0606054 (2006). https://doi.org/ 10.48550/arXiv.hep-ph/0606054. arXiv:hep-ph/0606054 [hep-ph]

    Pith/arXiv arXiv doi:10.48550/arxiv.hep-ph/0606054 2006

  80. [86]

    Barger, W.Y

    V. Barger, W.Y. Keung, G. Shaughnessy, A. Tregre, High energy neutrinos from neutralino annihilations in the Sun. Phys.Rev.D 76(9), 095008 (2007). https://doi.org/10. 1103/PhysRevD.76.095008. arXiv:0708.1325 [hep-ph]

    Pith/arXiv arXiv 2007

Showing first 80 references.